An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685

Bluhm, P.; Πάλλη, Ε.; Molaverdikhani, Karan; Kemmer, J.; Hatzes, A. P.; Kossakowski, D.; Stock, S.; Caballero, J. A.; Lillo-Box, J.; Béjar, V. J. S.; Soto, M. G.; Amado, P. J.; Brown, P. Lancaster; Cadieux, Charles; Cloutier, Ryan; Collins, Karen A.; Collins, Kevin I.; Cortés-Contreras, M.; Doyon, René; Dreizler, S.; Espinoza, N.; Fukui, A.; González-Álvarez, E.; Henning, Th.; Horne, K.; Jeffers, S. V.; Jenkins, Jon M.; Jensen, Eric L. N.; Kaminski, A.; Kielkopf, John F.; Kusakabe, Nobuhiko; Kuerster, M.; Lafrenière, David; Luque, R.; Murgas, F.; Montes, D.; Morales, J. C.; Narita, Norio; Passegger, V. M.; Quirrenbach, A.; Schoefer, P.; Reffert, S.; Reiners, A.; Ribas, I.; Ricker, G.; Seager, Sara; Schweitzer, A.; Schwarz, Richard P.; Tamura, Motohide; Trifonov, T.; Vanderspek, R.; Winn, Joshua N.; Zechmeister, M.; Osorio, M. R. Zapatero

doi:10.1051/0004-6361/202140688

Cited by 35 publications

(21 citation statements)

References 103 publications

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“…Their resulting RV semiamplitude is discrepant from ours at 5σ as they measure a larger RV semiamplitude of =  K 10.8 1.0 m s −1 and show that TOI-1634 b is likely consistent with an Earth-like composition. Similarly, the second USP planet presented in Hirano et al (2021;TOI-1685 b) was also found to be consistent with an Earth-like composition, whereas this planet was previously shown to be underdense relative to an Earth-like composition using CARMENES RV measurements (Bluhm et al 2021). The similar analyses conducted in this work, in Hirano et al (2021), and in Bluhm et al (2021) suggest that the differences in the IRD results compared to HARPS-N for TOI-1634 b and compared to CARMENES for TOI-1685 b are derived from the IRD data and not from issues with any one group's analysis.…”

Section: An Independent Analysis Of the Toi-1634 Systemmentioning

confidence: 52%

“…Similarly, the second USP planet presented in Hirano et al (2021;TOI-1685 b) was also found to be consistent with an Earth-like composition, whereas this planet was previously shown to be underdense relative to an Earth-like composition using CARMENES RV measurements (Bluhm et al 2021). The similar analyses conducted in this work, in Hirano et al (2021), and in Bluhm et al (2021) suggest that the differences in the IRD results compared to HARPS-N for TOI-1634 b and compared to CARMENES for TOI-1685 b are derived from the IRD data and not from issues with any one group's analysis. The exact cause of these discrepancies is currently unknown, and their resolution is left as a future exercise.…”

Section: An Independent Analysis Of the Toi-1634 Systemmentioning

confidence: 52%

“…51 TOIs 198.01, 203.01, 256.01, 1266.02, 2094.01, and 2095.02. (0.5 M e ). This proposition is further supported by the composition of the other keystone USP planet in Figure 9: the sub-Neptune TOI-1685 b whose host stellar mass is nearly identical to that of TOI-1634 Bluhm et al 2021). However, because models of thermally driven mass loss have assumed that the underlying cores of the closein planet population are Earth-like, if TOI-1634 b is rocky but not Earth-like (i.e., Ca-and Al-enriched), then its mass and radius may still be consistent with models of thermally driven mass loss.…”

Section: Implications For the Emergence Of The Radius Valley Around Early M Dwarfsmentioning

confidence: 63%

“…Since its science operations began in 2018 July, NASA's Transiting Exoplanet Survey Satellite (TESS; Ricker et al 2015) has uncovered a wealth of transiting planet candidates whose orbital periods and radii lie within the radius valley, including three planets transiting early M dwarfs (TOI-1235 b; Bluhm et al 2020;Cloutier et al 2020b, TOI-776 b;Luque et al 2021, TOI-1685Bluhm et al 2021). Radius valley planets whose periods P and radii r p satisfy Cloutier & Menou 2020) are referred to as keystone planets and are valuable targets to conduct tests of the competing radius valley emergence models across a range of stellar masses.…”

Section: Introductionmentioning

confidence: 99%

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TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Cloutier

Charbonneau

Stassun

et al. 2021

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Section: An Independent Analysis Of the Toi-1634 Systemmentioning

confidence: 52%

Section: An Independent Analysis Of the Toi-1634 Systemmentioning

confidence: 52%

Section: Implications For the Emergence Of The Radius Valley Around Early M Dwarfsmentioning

confidence: 63%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Cloutier

Charbonneau

Stassun

et al. 2021

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“…We found the fluctuations are too small to be observable for an Earth-sized planet like Proxima Centauri b, but as QBOlike phenomena have also been detected on Jupiter and Saturn in the solar system (Showman et al 2019;Orton et al 1991;Leovy et al 1991), a LASO could potentially occur on a larger planet with greater potential for observation. This could be particularly important for short-period, potentially tidally locked, super-Earth or mini-Neptune-type planets detected by missions such as the Transiting Exoplanet Survey Satellite (see Bluhm et al (2021) for a recent example)…”

Section: Atmospheric Water Vapour Oscillationsmentioning

confidence: 99%

Longitudinally asymmetric stratospheric oscillation on a tidally locked exoplanet

Cohen,

Bollasina,

Palmer

et al. 2021

Preprint

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Using a three-dimensional general circulation model, we show that the atmospheric dynamics on a tidally locked Earth-like exoplanet, simulated with the planetary and orbital parameters of Proxima Centauri b, support a longitudinally asymmetric stratospheric wind oscillation (LASO), analogous to Earth's quasi-biennial oscillation (QBO). In our simulations, the LASO has a vertical extent of 35-55 km, a period of 5-6.5 months, and a peak-to-peak wind speed amplitude of -70 to +130 ms −1 with a maximum at an altitude of 41 km. Unlike the QBO, the LASO displays longitudinal asymmetries related to the asymmetric thermal forcing of the planet and to interactions with the resulting stationary Rossby waves. The equatorial gravity wave sources driving the LASO are localised in the deep convection region at the substellar point and in a jet exit region near the western terminator, unlike the QBO, for which these sources are distributed uniformly around the planet. Longitudinally, the western terminator experiences the highest wind speeds and undergoes reversals earlier than other longitudes. The antistellar point only experiences a weak oscillation with a very brief, low-speed westward phase. The QBO on Earth is associated with fluctuations in the abundances of water vapour and trace gases such as ozone which are also likely to occur on exoplanets if these gases are present. Strong fluctuations in temperature and the abundances of atmospheric species at the terminators will need to be considered when interpreting atmospheric observations of tidally locked exoplanets.

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A multi-planetary system orbiting the early-M dwarf TOI-1238

González-Álvarez

Osorio

Sanz-Forcada

et al. 2022

A&A

Self Cite

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Context. The number of super-Earth and Earth-mass planet discoveries has increased significantly in the last two decades thanks to the Doppler radial velocity and planetary transit observing techniques. Either technique can detect planet candidates on its own, but the power of a combined photometric and spectroscopic analysis is unique for an insightful characterization of the planets, which in turn has repercussions for our understanding of the architecture of planetary systems and, therefore, their formation and evolution. Aims. Two transiting planet candidates with super-Earth radii around the nearby (d = 70.64 ± 0.06 pc) K7–M0 dwarf star TOI-1238 were announced by NASA’s Transiting Exoplanet Survey Satellite (TESS), which observed the field of TOI-1238 in four different sectors. We aim to validate their planetary nature using precise radial velocities taken with the CARMENES spectrograph. Methods. We obtained 55 CARMENES radial velocity measurements that span the 11 months between 9 May 2020 and 5 April 2021. For a better characterization of the parent star’s activity, we also collected contemporaneous optical photometric observations at the Joan Oró and Sierra Nevada observatories and retrieved archival photometry from the literature. We performed a combined TESS+CARMENES photometric and spectroscopic analysis by including Gaussian processes and Keplerian orbits to account for the stellar activity and planetary signals simultaneously. Results. We estimate that TOI-1238 has a rotation period of 40 ± 5 d based on photometric and spectroscopic data. The combined analysis confirms the discovery of two transiting planets, TOI-1238 b and c, with orbital periods of 0.764597−0.000011+0.000013 d and 3.294736−0.000036+0.000034 d, masses of 3.76−1.07+1.15 M⊕ and 8.32−1.88+1.90 M⊕, and radii of 1.21−0.10+0.11 R⊕ and 2.11−0.14+0.14 R⊕. They orbit their parent star at semimajor axes of 0.0137 ± 0.0004 au and 0.036 ± 0.001 au, respectively.The two planets are placed on opposite sides of the radius valley for M dwarfs and lie between the star and the inner border of TOI-1238’s habitable zone. The inner super-Earth TOI-1238 b is one of the densest ultra-short-period planets ever discovered (ρ = 11.7−3.4+4.2 g cm−3). The CARMENES data also reveal the presence of an outer, non-transiting, more massive companion with an orbital period and radial velocity amplitude of ≥600 d and ≥70 m s−1, which implies a likely mass of M ≥ 2 √(1− e2) MJup and a separation ≥1.1 au from its parent star.

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An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685

Cited by 35 publications

References 103 publications

TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Longitudinally asymmetric stratospheric oscillation on a tidally locked exoplanet

A multi-planetary system orbiting the early-M dwarf TOI-1238

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